Types of Hot Jupiter Atmospheres

Бисикало, Д. В.; Kaygorodov, P. V.; Ionov, D. E.; Shematovich, V. I.

doi:10.1007/978-3-319-09749-7_5

Cited by 7 publications

(2 citation statements)

References 28 publications

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“…considerably larger than the lower limit of 4 R p determined by Lai et al (2010) using the F10 data. In the models of Bisikalo et al (2013bBisikalo et al ( ,a, 2014 and Cherenkov et al (2014), planets undergoing Roche lobe overflow exhibit either 'quasi-closed' or 'open' atmospheres, dependent on the rate of mass outflow from the planet. For WASP-12b the prominence of a quasiclosed atmosphere could extend to 15-30 R p depending on the shape of the outflowing stream, although this would require extremely low stellar wind speeds (of order 10 km s −1 ).…”

Section: Discussionmentioning

confidence: 99%

“…2 in F10). To date there are two main hypotheses put forward to explain the claimed early ingress in the transit of WASP-12b: (a) material of planetary origin overflowing the Roche lobe at the L-1 point and deflecting in the direction of planetary motion (Lai et al 2010;Bisikalo et al 2013bBisikalo et al ,a, 2014Cherenkov et al 2014), and (b) shocked material in a magnetosheath upstream (with respect to the planet's orbit) of the planet's magnetosphere (Lai et al 2010;Vidotto et al 2010;Vidotto et al 2011b,a;Llama et al 2011;Alexander et al 2015), although the data were unable to distinguish between these two scenarios. The second visit, presented by H12, also exhibited low fluxes at pre-transit phases out to φ 0.83, although there were significant differences between the values obtained in the first and second visits at similar phases.…”

Section: Introductionmentioning

confidence: 99%

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HUBBLE SPACE TELESCOPEOBSERVATIONS OF THE NUV TRANSIT OF WASP-12b

Nichols

Wynn

Goad

et al. 2015

ApJ

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We present new observations of four closely-spaced NUV transits of the hot Jupiter-like exoplanet WASP-12b using HST/COS, significantly increasing the phase resolution of the observed NUV light curve relative to previous observations, while minimising the temporal variation of the system. We observe significant excess NUV absorption during the transit, with mean normalised in-transit fluxes of F norm 0.97, i.e. 2-5 σ deeper than the optical transit level of 0.986 for a uniform stellar disk (the exact confidence level depending on the normalisation method used). We further observe an asymmetric transit shape, such that the post-conjunction fluxes are overall 2-3 σ higher than pre-conjunction values, and characterised by rapid variations in count rate between the pre-conjunction and out of transit levels. We do not find evidence for an early ingress to the NUV transit as suggested by earlier HST observations. However, we show that the NUV count rate observed prior to the optical transit is highly variable, but overall 2.2-3.0 σ below the post-transit values and comparable in depth to the optical transit, possibly forming a variable region of NUV absorption from at least phase φ 0.83, limited by the data coverage. Subject headings: planets and satellites: atmospheres -planets and satellites: individual (WASP-12b)planets and satellites: magnetic fields -planet-star interactions -ultraviolet: planetary systems

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

HUBBLE SPACE TELESCOPEOBSERVATIONS OF THE NUV TRANSIT OF WASP-12b

Nichols

Wynn

Goad

et al. 2015

ApJ

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The estimate of hot Jupiter mass loss rate in the interaction with CME from a solar type star

2015

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Abstract. We consider the influence of a coronal mass ejection (CME) of a solar type star on the mass loss rate of a hot Jupiter exoplanet. We have conducted 3D numerical gas-dynamic simulations of the planet's atmosphere that interacts with CME. Using the results of these simulations we have estimated the specific parameters that influence the mass loss rate. Based on the assumption that CME totally sweeps away part of the planet's gaseous envelope located outside the Roche lobe we estimated the maximum mass loss rate. Finally, we have considered the dependence of mass loss rate on the frequency of CMEs in course of star's evolution.

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